%0 Generic %1 vogelsberger2013physical %A Vogelsberger, Mark %A Genel, Shy %A Sijacki, Debora %A Torrey, Paul %A Springel, Volker %A Hernquist, Lars %A ), %D 2013 %K arepo cosmological simulation %T A physical model for cosmological simulations of galaxy formation %U http://arxiv.org/abs/1305.2913 %X We present a new comprehensive model of the physics of galaxy formation designed for large-scale hydrodynamical simulations of structure formation using the moving mesh code AREPO. Our model includes primordial and metal line cooling with self-shielding corrections, stellar evolution and feedback processes, gas recycling, chemical enrichment, a novel subgrid model for the metal loading of outflows, black hole (BH) seeding, BH growth and merging procedures, quasar- and radio-mode feedback, and a prescription for radiative electro-magnetic (EM) feedback from active galactic nuclei (AGN). Stellar feedback is realised through kinetic outflows. The scaling of the mass loading of galactic winds can be set to be either energy or momentum driven, or a mixture of both. The metal mass loading of outflows can be adjusted independently of the wind mass loading. This is required to simultaneously reproduce the stellar mass content of low mass haloes and their gas oxygen abundances. Radiative EM AGN feedback is implemented assuming an average spectral energy distribution and a luminosity-dependent scaling of obscuration effects. This form of feedback suppresses star formation more efficiently than continuous thermal quasar-mode feedback alone, but is less efficient than mechanical radio-mode feedback in regulating star formation in massive haloes. We contrast simulation predictions for different variants of our model with observations. We identify a best match model and show that it reproduces, among other things, the cosmic star formation history, the stellar mass function, the stellar mass - halo mass relation, SDSS galaxy luminosity functions, and the Tully-Fisher relation. We can achieve this success only if we invoke very strong forms of stellar and AGN feedback. In particular, the strength of radio-mode feedback needs to be increased significantly compared to previous studies.Abridged

@misc{vogelsberger2013physical, abstract = {We present a new comprehensive model of the physics of galaxy formation designed for large-scale hydrodynamical simulations of structure formation using the moving mesh code AREPO. Our model includes primordial and metal line cooling with self-shielding corrections, stellar evolution and feedback processes, gas recycling, chemical enrichment, a novel subgrid model for the metal loading of outflows, black hole (BH) seeding, BH growth and merging procedures, quasar- and radio-mode feedback, and a prescription for radiative electro-magnetic (EM) feedback from active galactic nuclei (AGN). Stellar feedback is realised through kinetic outflows. The scaling of the mass loading of galactic winds can be set to be either energy or momentum driven, or a mixture of both. The metal mass loading of outflows can be adjusted independently of the wind mass loading. This is required to simultaneously reproduce the stellar mass content of low mass haloes and their gas oxygen abundances. Radiative EM AGN feedback is implemented assuming an average spectral energy distribution and a luminosity-dependent scaling of obscuration effects. This form of feedback suppresses star formation more efficiently than continuous thermal quasar-mode feedback alone, but is less efficient than mechanical radio-mode feedback in regulating star formation in massive haloes. We contrast simulation predictions for different variants of our model with observations. We identify a best match model and show that it reproduces, among other things, the cosmic star formation history, the stellar mass function, the stellar mass - halo mass relation, SDSS galaxy luminosity functions, and the Tully-Fisher relation. We can achieve this success only if we invoke very strong forms of stellar and AGN feedback. In particular, the strength of radio-mode feedback needs to be increased significantly compared to previous studies.[Abridged]}, added-at = {2013-05-15T19:13:48.000+0200}, author = {Vogelsberger, Mark and Genel, Shy and Sijacki, Debora and Torrey, Paul and Springel, Volker and Hernquist, Lars and )}, biburl = {https://www.bibsonomy.org/bibtex/20a6fad1bb96cc44634a5a904b0a1d6e8/miki}, description = {[1305.2913] A physical model for cosmological simulations of galaxy formation}, interhash = {f150740d0d59e316aae956cfdca6e433}, intrahash = {0a6fad1bb96cc44634a5a904b0a1d6e8}, keywords = {arepo cosmological simulation}, note = {cite arxiv:1305.2913Comment: 38 pages, 16 figures, submitted to MNRAS. Volume-rendering movies and high-resolution images can be found at http://www.cfa.harvard.edu/itc/research/arepogal/}, timestamp = {2013-05-15T19:13:48.000+0200}, title = {A physical model for cosmological simulations of galaxy formation}, url = {http://arxiv.org/abs/1305.2913}, year = 2013 }